Extract green and red lines that we haven't got yet from PZ cube

Load up the cube, as per previous notebooks.

Get all the regions from previous notebooks:

Start with the green range

So in this version we do not have the mcube

Extract He I 5875 line

No need to fix sky

This shows exatly the same 3 clumps in the I-V plane as we see in the H lines. But the sigma behavior is more homogeneous, with no evidence that sigma varies with anything.

I think this line is a triplet, so it may be that the sigma has a contribution from the fine structure splitting.

Extract [Cl III] lines

Extract [N II] line

Second, the red range

The [Ar IV] auroral lines

So subtracting the median spectrum is vital with the PZ cube. With the subtraction (blue line) we get a reasonable spectrum that is very similar to the one from the ESO cube.

But without the median subtraction (orange line) we get a complete mess

Left to right

Also lots of sky lines

Time to break out the median-subtracted cube I guess

So this is pretty good. The maps are just as good as the ESO cube ones.

7263 is the best, and 7171 is tolerable, but more affected by stellar sources. 7237 is blended with both a sky line and a DRL, so it is a lot messier

The [Cl IV] 7531 line

This looks really good

The [Ar III] 7136 line

This one is so bright (and evenly spread over the nebula) that we should not use the median-subtracted cube

This is the best example yet for the kinematics. Everything is sharpened up a bit, as compared with the H and He lines. We now see that there are clearly 4 different clumps in the I-V plane. Also, there are weak negative trends of sigma with I and V

Even better with the 4x4 binning. And this is also far better than what we got with the ESO cube, so this is a case whwre the PZ cube offers a clear advantage.

Third, the far-red range

We just go as var as the Paschen limit, since there is no point fitting a polynomial across an ionization edge.

Look at the far red range for interesting bow shock lines

There is nothing much interesting in this range. Lots of weak He I lines. There are also a lot of low ionization lines, ssuch as Ca I], which I might want to come back to later.

This has the [Cl IV] 8045.62 line, although it is blended with a lower ionization line.

We can see a clear contamination by something coming from the filaments.

Fourth and finally, the infrared range

Those continuum fits are not great, but apatr from the brown spectrum they are acceptable

Look at what we have got for the bow shock in the infrared range

Mostly H lines

The [S III] line and the brightest H line are all we need for the bow shock really. We could grab the [C I] line too though.

The [S III] 9069 line

These are very good again, similar to [Ar III], although this time we can also see a different V for the very brightest pixels (MYSO C), which is like 161 km/s.

Also, we don't see the negative trend of sigma with brightness here, which makes me think that wnat we saw in [Ar III] might have been due to an unrecognised blend.